http://arxiv.org/abs/1807.04755
We have studied the long-term evolution of star clusters of the solar neighborhood, starting from their birth in gaseous clumps until their complete dissolution in the Galactic tidal field. We have combined the “local-density-driven cluster formation model” of Parmentier & Pfalzner (2013) with direct N-body simulations of clusters following instantaneous gas expulsion.
We have studied the relation between cluster dissolution time, $t_{dis}$, and cluster “initial” mass, $M_{init}$, defined as the cluster {mass at the end of the dynamical response to gas expulsion (i.e. violent relaxation), when the cluster age is 20-30 Myr}. We consider the “initial” mass to be consistent with other works which neglect violent relaxation. The model clusters formed with a high star formation efficiency (SFE — i.e. gas mass fraction converted into stars) follow a tight mass-dependent relation, in agreement with previous theoretical studies. However, the low-SFE models present a large scatter in both the “initial” mass and the dissolution time, and a shallower mass-dependent relation than high-SFE clusters. Both groups differ in their structural properties on the average. Combining two populations of clusters, high- and low-SFE ones, with domination of the latter, yields a cluster dissolution time for the solar neighborhood in agreement with that inferred from observations, without any additional destructive processes such as giant molecular cloud encounters.
An apparent mass-independent relation may emerge for our low-SFE clusters when we neglect low-mass clusters (as expected for extra-galactic observations), although more simulations are needed to investigate this aspect.
B. Shukirgaliyev, G. Parmentier, A. Just, et. al.
Mon, 16 Jul 18
16/55
Comments: Acceped for publication in Astrophysical Journal (ApJ), 17 pages, 9 figures